2008/06/01 by Ken'ichi Nomoto, K. Nomoto, Shinya Wanajo +3 · 1 citation
Physics and Astronomy · #Gamma-ray bursts and supernovae #Pulsars and Gravitational Waves Research #Stellar, planetary, and galactic studies #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1017/s1743921308027816
published as IAU Symposium No. 254 "The Galaxy Disk in Cosmological Context" (2009), eds. J. Andersen, J. Bland-Hawthorn, and B. Nordstrom (Cambridge University Press) · 13 pages, 10 figures. Published in the Proceedings of IAU Symposium No. 254 "The Galaxy Disk in Cosmological Context" (2009), eds. J. Andersen, J. Bland-Hawthorn, and B. Nordstrom (Cambridge University Press), pp. 355-367
openalex publication_date 2008/06/01 · arxiv created 2009/05/14 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/04
Abstract We review the final stages of stellar evolution, supernova properties, and chemical yields as a function of the progenitor's mass. (1) 8 - 10 M ⊙ stars are super-AGB stars when the O+Ne+Mg core collapses due to electron capture. These AGB-supernovae may constitute an SN 2008S-like sub-class of Type IIn supernovae. These stars produce little α-elements and Fe-peak elements, but are important sources of Zn and light p-nuclei. (2) 10 - 90 M ⊙ stars undergo Fe-core collapse. Nucleosynthesis in aspherical explosions is important, as it can well reproduce the abundance patterns observed in extremely metal-poor stars. (3) 90 - 140 M ⊙ stars undergo pulsational nuclear instabilities at various nuclear burning stages, including O and Si-burning. (4) Very massive stars with M ≳ 140 M ⊙ either become pair-instability SNe, or undergo core-collapse to form intermediate mass black holes if the mass loss is small enough.